From Gamma-Ray Bursts/Hypernovae To Black-Hole Binaries

TL;DR

This paper presents a binary stellar evolution model that links gamma-ray bursts, hypernovae, and black-hole binaries, highlighting the role of angular momentum transfer and black hole energy extraction mechanisms.

Contribution

It introduces a detailed evolutionary pathway connecting long gamma-ray bursts and hypernovae to black-hole binary formation, emphasizing the impact of mass transfer and tidal spin-up.

Findings

The model successfully reproduces observed properties of black-hole binaries.

Black-hole spin and energy extraction via the Blandford-Znajek mechanism are key to GRB/HN production.

Predicted black-hole binary characteristics align with observed systems.

Abstract

In this work I summarize a model of binary stellar evolution involving Case C mass transfer followed by a common envelope that strips away the hydrogen from the core of the primary star at the cost of shrinking the orbital separation and then, through tidal interaction, spins it up. This model is then used to produce the possible progenitors of long gamma-ray burst / hypernova (GRB/HN) explosions. As the core collapses with the newly supplied angular momentum it produces a Kerr black hole surrounded by an accretion disk. Energy is extracted from the rotation of the black hole (BH) through the Blandford-Znajek (BZ) mechanism to power both, the long gamma-ray burst and the accompanying hypernova (supernova type Ic broad line). If the binary survives the asymmetric mass loss its remnant is a black-hole binary that may eventually be observed as a soft X-ray transient (SXT) when the companion evolves and starts to transfer mass back to the black hole. A comparison with a sample of black-hole binaries where the masses and orbital periods are well constrained is performed.